Effects of σ* and φ on the proto-neutron star PSR J0348+0432

  • The influence of σ* and φ on the proto-neutron star (PNS) PSR J0348+0432 is described by the relativistic mean field theory (RMFT) through choosing effective coupling constants. We use an entropy per baryon S=1 to describe the thermal effects on PSR J0348+0432 in this work and compare this PNS with and without σ*, φ. These effects include the particle number distribution, mass-radius relation, moment of inertia and surface gravitational redshift. The PNS PSR J0348+0432 with σ* and φ has more nucleons and will push forward the threshold for the appearance of the hyperons. The mass-radius relations are (2.010M, 12.6520 km) with σ* and φ and (2.010M, 12.6170 km) without σ* and φ. The moments of inertia corresponding to PNS PSR J0348+0432 are (2.010M, 1.510×1045 g·cm2) and (2.010M, 1.559×1045 g·cm2) respectively, and the surface gravitational redshifts are (2.010M, 0.3747) and (2.010M, 0.3701) respectively. With the help of these calculations, we study the restriction of σ* and φ on the interactions between baryons in the PNS core.
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  • [1] B. P. Abbott et al, Phys. Rev. Lett., 119:161101 (2017)
    [2] D. A. Coulter, R. J. Foley, C. D. Kilpatrick, M. R. Drout, A. L. Piro, B. J. Shappee, M. R. Siebert, J. D. Simon, N. Ulloa, D. Kasen, B. F. Madore, A. Murguia-Berthier, Y.-C. Pan, J. X. Prochaska, E. Ramirez-Ruiz, A. Rest, and C. Rojas-Bravo, Science, 358:1556 (2017)
    [3] P. B. Demorest, T. Pennucci, and S. M. Ransom et al, Nature(London), 467:1081 (2010)
    [4] J. Antoniadis, P. C. C. Freire et al, Science, 340:448 (2013)
    [5] B. Hong, H. Y. Jia, X. L. Mu, and X. Zhou, Chin. Phys. C, 40:065101 (2016)
    [6] Prasanta Char and Sarmistha Banik, Phys. Rev. C, 90:015801 (2014)
    [7] Feryal zel, Dimitrios Psaltis et al, Astrophys. J. Lett., 724:L199-L202 (2010)
    [8] Z. Zhang, L. W. Chen, Phys. Rev. C, 94:064326 (2016)
    [9] Ritam Mallick, Phys. Rev. C, 87:025804 (2013)
    [10] Q. F. Xiang, W. Z. Jiang, D. R. Zhang, and R. Y. Yang, Phys. Rev. C, 89:025803 (2014)
    [11] L. Ang et al, Chin. phys, 16:1934 (2007)
    [12] J. Schaffner, C. B. Dover, A. Gal, C. Greiner, and H. Stcker, Phys. Rev. Lett., 71:1328 (1993)
    [13] H. Zheng, L. W. Chen, Phys. Rev. D, 85:043013 (2012)
    [14] S. Gandolfi, J. Carlson, and Sanjay Reddy, Phys. Rev. C, 85:032801 (2012)
    [15] Y. Sugahara, H. Toki, Nucl. Phys. A, 579:557 (1994)
    [16] X. F. Zhao, Phys. Rev. C, 92:055802 (2015)
    [17] Norman K. Glendenning, Phys. Rev. C, 23:2757 (1981)
    [18] M. M. Sharma, M. A. Nagarajan, P. Ring, Phys. Lett. B, 312:377 (1993)
    [19] W. Koepf, M. M. Sharma, P. Ring, Nucl. Phys. A, 533:95 (1991)
    [20] Z. Z. Ren, Phys. Rev. C, 65:051304 (2002)
    [21] J. Boguta, A. R. Bodmer, Nucl. Phys. A, 292:413 (1977)
    [22] J. Schaffner, C. B. Dover, A. Gal, C. Greiner, D. J. Millener, and H. Stcker, Ann. Phys., 235:35 (1994)
    [23] Madappa Prakash, Ignazio Bombaci, Manju Prakash, Paul J. Ellis, James M. Lattimer, and Roland Knorren, Phys. Reps., 280:1 (1997)
    [24] J. R. Oppenheimer, and G. M. Volkoff, Phys. Rev., 55:374 (1939)
    [25] F. J. Fattoyev, and J. Piekarewicz, Phys. Rev. C, 82:025810 (2010)
    [26] Lee Lindblom, Astrophys. J., 278:364 (1984)
    [27] Benjamin D. Lackey, Mohit Nayyar, and Benjamin J. Owen, Phys. Rev. D, 73:024021 (2006)
    [28] N. K. Glendenning, Astrophys. J., 293:470 (1985)
    [29] S. Weissenborn, D. Chatterjee, and J. Schaffner-Bielich, Nucl. Phys. A, 881:62 (2012)
    [30] D. J. Millener, C. B. Dover, and A. Gal, Phys. Rev. C, 38:2700 (1988)
    [31] J. Schaffner, C. Greiner, and H. Stcker, Phys. Rev. C, 46:322 (1992)
    [32] C. J. Batty, E. Friedman, and A. Gal, Phys. Reps., 287:385 (1997)
    [33] J. Schaffner-Bielich, A. Gal, Phys. Rev. C, 62:034311 (2000)
    [34] S. Aoki, S. Y. Bahk, K. S. Chung et al, Phys. Lett. B, 355:45 (1995)
    [35] P. Khaustov, D. E. Alburger et al, Phys. Rev. C, 61:054603 (2000)
    [36] N. K. Glendenning and S. A. Moszkowski, Phys. Rev. Lett., 67:2414 (1991)
    [37] S. Pal, M. Hanauske, I. Zakout, H. Stcker, and W. Greiner, Phys. Rev. C, 60:015802 (1999)
    [38] X. L. Mu, H. Y. Jia, X. Zhou, and H. Wang, Astrophys. J, 846:140 (2017)
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Bin Hong and Zhong-Zhou Ren. Effects of σ* and φ on the proto-neutron star PSR J0348+0432[J]. Chinese Physics C, 2018, 42(8): 084105. doi: 10.1088/1674-1137/42/8/084105
Bin Hong and Zhong-Zhou Ren. Effects of σ* and φ on the proto-neutron star PSR J0348+0432[J]. Chinese Physics C, 2018, 42(8): 084105.  doi: 10.1088/1674-1137/42/8/084105 shu
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Received: 2018-05-03
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    Supported by National Natural Science Foundation of China (11535004, 11761161001) and the National Major State Basic Research and Development Program of China (2016YFE0129300)

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Effects of σ* and φ on the proto-neutron star PSR J0348+0432

  • 1.  Department of Physics, Nanjing University, Nanjing 210008, China
  • 2. Department of Physics, Nanjing University, Nanjing 210008, China
  • 3. School of Physics Science and Engineering, Tongji University, Shanghai 200092, China
Fund Project:  Supported by National Natural Science Foundation of China (11535004, 11761161001) and the National Major State Basic Research and Development Program of China (2016YFE0129300)

Abstract: The influence of σ* and φ on the proto-neutron star (PNS) PSR J0348+0432 is described by the relativistic mean field theory (RMFT) through choosing effective coupling constants. We use an entropy per baryon S=1 to describe the thermal effects on PSR J0348+0432 in this work and compare this PNS with and without σ*, φ. These effects include the particle number distribution, mass-radius relation, moment of inertia and surface gravitational redshift. The PNS PSR J0348+0432 with σ* and φ has more nucleons and will push forward the threshold for the appearance of the hyperons. The mass-radius relations are (2.010M, 12.6520 km) with σ* and φ and (2.010M, 12.6170 km) without σ* and φ. The moments of inertia corresponding to PNS PSR J0348+0432 are (2.010M, 1.510×1045 g·cm2) and (2.010M, 1.559×1045 g·cm2) respectively, and the surface gravitational redshifts are (2.010M, 0.3747) and (2.010M, 0.3701) respectively. With the help of these calculations, we study the restriction of σ* and φ on the interactions between baryons in the PNS core.

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